Conclusions of the 16-17 September 1999 meeting -------------------------------- 1. Main tasks for Kiruna flight -------------------------------- Fast Stellar Sensor: Decision to put a red filter to work with sunrise awaits further star sensor data reduction. Add a magnetometer to have 1 degree precision as a backup of FSS during sun periods: No Add a sun sensor, 1' accuracy : yes, as a backup tool for pointing measurements during day (sun below 10 degree elevation) Need End-to-end Optical simulation of Trapani and Kiruna configurations (primary-secondary-horns) Use 4K bolometers to map the horns alone. Upgrade ground-based optical calibration tools to test the Kiruna flight optical configuration: main beam with chopper with reticule attached Use Gunn diode for sidelobes Buy new GPS Inmarsat and TM/TC at Kiruna New mirrors for Archeops: Study needed New gondola design to save weight Fix the cryostat leak Change bolometer connectors and possibly JFETs Photometric data on the web Cross-checking bolometer calibrations between QMW and CRTBT Solve for the (small) failures of the on-board data recorder and upgrade to 2 GByte Organise coodination with CNES for Kiruna Goals of Kiruna 2001: Primary: Measure C_l on the broadest range of l with emphasis on low l. Secondary: 1) Make large (sub)mm maps. 2) Measure the polarised radiation of interstellar dust. Subset of bolometers and horns delivered for 1st April 2000 Add a blind bolometer: ? Nominal detector configuration for Kiruna agreed at the meeting: Freq (GHz) Number of bolometers beam (arcmin) Polarisation 143 8 7 no 217 8 5 no 350 6 5 yes 545 2 5 no with new corrugated flared horn design ------------------------------------------------------------ Software for data reduction ------------------------------------------------------------ - Software in a CVS repository, temporarily on cheops - Cross checking the different available softwares - First cut at global processing, to understand the needs of the various stages - Here is a list of identified tasks with a non-exhaustive share between the different institutes Level 1: extract signal and pointing information from the raw data TOI improvements: CEA Fast Stellar Sensor: LAL, Roma Level 2: timeline treatment Noise analysis and parasitic signals: CdF, IAS, OMP, ISN, QMW Glitches: IAS Calibration: CdF, LAOG, CRTBT, QMW photometric model, optical calculations, bolometer behaviour... Level 3: Map making Map reconstruction (Healpix and others): IAP, CdF, OMP Submap projector and map tools: IAS, IAP Ephemerids and point sources: IAP, ISN External data handling (COBE, IRAS...): IAS, Level4: Extracting science Correlation function and C_l estimators: UMinn, CdF, IAP Noise correlation and Matrix estimators: OMP, ISN Science from C_l Separation of components: IAP